adsabs/AstroCLIMB huggingface dataset:
Paper: Unusual Abundances from Planetary System Material Polluting the White Dwarf G238-44
Authors: Ted M Johnson, Beth L. Klein, D. Koester, Carl Melis, B. Zuckerman, M. Jura
Figure caption: Multiple epochs of HIRES spectra showing Ca II K (left) and Mg II λ4481 (right). With the exception of the anomalous 2016 epoch, the line strengths all look the same over the 24 yr period during which the spectra were obtained.
Paper: Unusual Abundances from Planetary System Material Polluting the White Dwarf G238-44
Authors: Ted M Johnson, Beth L. Klein, D. Koester, Carl Melis, B. Zuckerman, M. Jura
Figure caption: Select regions of FUSE and HST spectra; the model with the best-fit abundances is overplotted in red. The STIS spectrum (showing the 2800 Å Mg II lines and 2600 Å Fe II lines) has been smoothed with a 5 pixel boxcar function.
Paper: Unusual Abundances from Planetary System Material Polluting the White Dwarf G238-44
Authors: Ted M Johnson, Beth L. Klein, D. Koester, Carl Melis, B. Zuckerman, M. Jura
Figure caption: Distribution of heliocentric radial velocities measured for the absorption lines detected in spectra of G238-44. See also Section 3.2.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: Parallax fitting for MF1 with VERA astrometry. Top panel: an example of the fitted parallax curve using the data points during the period 2019.8–2021.3 without an acceleration. Bottom left panel: residuals of the fitting using the data points during the period 2019.8–2021.3. The data points from the fitting including an acceleration have a constant horizontal offset from those without an acceleration for clarity. Bottom right panel: same as the bottom left panel, but for the period 2020.2–2021.3.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: Integrated flux curves of 22 GHz H2O masers from the cross-power (red circles) and total-power (green circles) spectra of the KVN and V-band optical light curve (blue stars) from the AAVSO monitoring data. The total-power spectra are using the weighted average of three KVN antennas (Kt, Ky, Ku), while the cross-power spectra are using the short baselines as shown in Figure 1. The V LSR velocity range for estimating the integrated flux densities is from −16 to −7 km s−1 and from 7 to 10 km s−1. At K band, the beam size of the KVN single-dish telescope is ∼130 arcseconds and the synthesized beam size of the projected Ky-Ku baseline is ∼11 mas for BX Cam. The black solid line shows the sinusoidal fit to the optical light curve with a period of 440 days.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: Left to right: moment-zero maps of the water maser emission in BX Cam from KVN, VERA, and EAVN (KVN+VERA+T6) observations at the same epoch, 2020 January 10. The maps are from images created by collapsing each spectral line cube to a single plane using the AIPS task SQASH, taking the weighted averages of each pixel. An ellipse in the lower left corner of each panel indicates the synthesized beam pattern of the image synthesis. The contour map is drawn with contour levels of 3, 6, 12, 24, … × σ, where 1σ corresponds to 0.03 Jy beam−1 (KVN), 0.04 Jy beam−1 (VERA), and 0.03 Jy beam−1 (EAVN), respectively.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: Registered map of the H2O and SiO (v = 1, J = 1 → 0) masers observed on 2020 January 10 using the KVN data, which were taken from velocity-channel integration with weights based on the rms noise level. The black star indicates the estimated position of the star at the center of the SiO maser ring using the least-squares circle method (Yoon et al. 2018). The red star indicates the position of the star derived from Gaia EDR3. The contour map is drawn with contour levels of 3, 6, 12, 24, … × σ, where 1σ corresponds to 0.025 Jy beam−1 (H2O) and 0.120 Jy beam−1 (SiO).
Paper: Monte Carlo Simulations on Possible Collimation Effects of Outflows to Fan Beam Emission of Ultraluminous Accreting X-Ray Pulsars
Authors: X. Hou, Y. You, L. Ji, R. Soria, S. N. Zhang, M. Y. Ge, L. Tao, S. Zhang, H. Feng, M. Zhou, Y. L. Tuo, L. M. Song, J. C. Wang
Figure caption: Collimation factor as a function of observing inclination angle, for different orientation angles Θ of the AC. In all cases, v is fixed to 0.1c. The calculated collimation factors (see text for details) are drawn in dashed lines and the collimation factors directly from simulation results are drawn in solid lines.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: EAVN images of the spatial structures of maser features (top left), with a zoom-in of the colored blocks (top right, bottom left, bottom right), observed on 2020 January 10 (ϕ = 2.00). These images are obtained after component fitting from the image data cube with AIPS task SAD. Each of the filled circles shows a velocity component (maser spot), and each maser feature (MF#) has a velocity-channel spacing of 0.105 km s−1. The position reference feature (MF1) is around the map origin.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: The cross-power H2O maser spectra on the Ky–Ku baseline (305 km). Few epochs are on the Ky–Kt baseline (476 km) when Ku is not available. Data from all 37 epochs were used.
Paper: The Astrometric Animation of Water Masers toward the Mira Variable BX Cam
Authors: Shuangjing Xu, Hiroshi Imai, Youngjoo Yun, Bo Zhang, María J. Rioja, Richard Dodson, Se-Hyung Cho, Jaeheon Kim, Lang Cui, Andrey M. Sobolev, James O. Chibueze, Dong-Jin Kim, Kei Amada, Jun-ichi Nakashima, Gabor Orosz, Miyako Oyadomari, Sejin Oh, Yoshinori Yonekura, Yan Sun, Xiaofeng Mai, Jingdong Zhang, Shiming Wen, Taehyun Jung
Figure caption: VERA image of J0524+7034 observed on 2020 January 10. The contour map is drawn with contour levels of 3, 6, 12, 24, … × σ, where 1σ corresponds to 0.005 Jy beam−1.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Normalized histograms of the residuals (data minus model) at each passband for Perseus E. These are fit with Gaussians to quantify the offset and dispersion (inset labels). Three different versions are shown in the top row. Left: (I  ν  − I  ν,m ) in MJy sr−1. Middle: (I  ν  − I  ν,m )/I  ν . Right: (I  ν  − I  ν,m )/σ  ν . In the lower row are the χ 2 map, the union mask with defining contour overlaid on the 250 μm intensity map, and the distribution function of ﹩\mathrm{log}({\chi }^{2})﹩. In the latter, the black line is the theoretical distribution function for k = 2. The brown histogram is the distribution for the entire map, whereas the cyan and tan histograms are for the union mask and complementary pixels outside the union mask, respectively.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Normalized histograms of ﹩\mathrm{log}(\tau )﹩ and T for the Perseus E region. The solid blue histograms are from HOTT while the blue-line histograms are from a run with β fixed to the median value in the common science region. The red-line histograms show the larger systematic changes for a fixed β of 2. Histograms from HGBS (cyan) and HP2 (tan) are also shown.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Like Figure 13, but for SED fits after tweaking the zero levels (Section 10.3). This plot is available in the online archive for all fields.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Left: map of the radiance of dust in Perseus E calculated from the parameters of the modified blackbody thermal dust model. Right: the χ 2 map, with a contour outlining the masked pixels.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Left: τ HOTT  of Perseus E. Right: T HOTT of Perseus E.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Histogram of the means of (I  ν  − I  ν,m )/I  ν  for all fields.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: 2D histogram of fractional uncertainty of τ HOTT  with respect to fractional uncertainty of T HOTT for Perseus E.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Left: uncertainty of τ HOTT  of Perseus E. Right: uncertainty of T HOTT of Perseus E.
Paper: Herschel Optimized Tau and Temperature (HOTT) Maps: Uncertainty Analysis and Robust Parameter Extraction
Authors: Ayushi Singh, Peter G. Martin
Figure caption: Fractional error of T HOTT of Perseus E.
Paper: Central Star Formation in Early-type Galaxy I Zw 81 in the Bootes Void
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan, Sugata Kaviraj
Figure caption: UVIT, FUV, and NUV images of the galaxy in the left and right panels, respectively. The color bar represents the flux and surface brightness distribution on the image. The 3σ limiting surface brightness values for FUV and NUV observation are 27.37 mag arcsec−2 and 27.92 mag arcsec−2, respectively. White contour represents the boundary of the galaxy seen in the optical wave band, whereas blue and cyan colored circles show the central region of the galaxy (r = 1.5″) and the outer radius of the ring (r = 4.2″). The star-forming clumps C1 and C2 are enclosed in a white open circle of radius 1″ each.
Paper: Central Star Formation in Early-type Galaxy I Zw 81 in the Bootes Void
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan, Sugata Kaviraj
Figure caption:  M ⋆ vs. sSFR distribution for void galaxies. The black star marker denotes IZw81. Black open circles are void galaxies with M ⋆ > 5 × 1010 M ⊙(Pan et al. 2012). The background galaxies (gray dots) are taken from Salim et al. (2016). The figure is divided into three sections: star-forming region (﹩\mathrm{log}s\mathrm{SFR}\geqslant -10.8﹩), green valley region (﹩-10.8\gt \mathrm{log}s\mathrm{SFR}\gt -11.8﹩), and quenched region (﹩\mathrm{log}s\mathrm{SFR}\leqslant -11.8;﹩ Barway & Saha 2020).
Paper: Central Star Formation in Early-type Galaxy I Zw 81 in the Bootes Void
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan, Sugata Kaviraj
Figure caption: Best-fit SEDs (fracAGN = 0./0.1) of I Zw 81 produced by CIGALE. The input broadband fluxes are marked with blue circles. The best-fit parameters can be found in Table 2. The error bars on the measured fluxes denote 1σ error bar. The filter response curves are shown in the figure with different colors.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: The visible light curve of nova V5856 Sgr/2016 taken from photometric data. The top plot shows the flattening of the decline that leaves the visible brightness nine magnitudes above its pre-outburst level of I > 22 (Munari et al. 2017), determined from pre-outburst ASASSN observations. The bottom curve shows a finer grid of dates that display the deliberate, slow steady rise and fall of the nova from its discovery, through visible maximum.
Paper: V5856 Sagittarii/2016: Broad Multiepoch Spectral Coverage of a Sustained High-luminosity Nova
Authors: Robert Williams, Frederick M. Walter, Richard J. Rudy, Ulisse Munari, Paul Luckas, John P. Subasavage, Jon C. Mauerhan
Figure caption: A series of low-resolution spectra taken by Paul Luckas in the weeks following outburst. The initial spectrum was the basis for his determination of the nova as Fe II class, from the prominence of the Fe II multiplet 42. The nova quickly evolved to display absorption lines that became prominent at visual maximum. Shortly thereafter the spectrum transformed back into an emission spectrum similar to that it displayed at the time of discovery, although with broader lines reflecting higher gas velocities.
Paper: Central Star Formation in Early-type Galaxy I Zw 81 in the Bootes Void
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan, Sugata Kaviraj
Figure caption: A comparison between CFHT and SDSS g-band images of I Zw 81. The magenta-colored crescent segment, vertical, and horizontal boxes highlight the tidal tail-like feature identified in CFHT observation. The same regions are overlayed on SDSS g-band image.
Paper: Central Star Formation in Early-type Galaxy I Zw 81 in the Bootes Void
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan, Sugata Kaviraj
Figure caption: CFHT g−r color map of I Zw 81. The colors shown are not corrected for Galactic or internal extinction. The black solid ellipse traces the GALFIT modeled bar (r e = 0.″92, θ P.A. = 45° q = 0.55) whereas the radius of the black dotted circle denotes r break(= 4.″2).
Paper: Central Star Formation in Early-type Galaxy I Zw 81 in the Bootes Void
Authors: Divya Pandey, Kanak Saha, Ananta C. Pradhan, Sugata Kaviraj
Figure caption:  M ⋆ vs. sSFR distribution for a sample of S0, barred S0, and barred Sy2 S0 galaxies. The S0 sample is taken from Nair & Abraham (2010).
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: Calculated disk radius as a function of disk inclination. Different colors indicate different targets. Dashed and solid lines represent the radius calculated with the best-fit rotational velocity of optical and NIR lines (Table 7), respectively. The circles represent the radius calculated with inclinations of 30°, 45°, 60°, and 90°.
Paper: Photometric and Spectroscopic Study of the EXor-like Eruptive Young Star Gaia19fct
Authors: Sunkyung Park, Ágnes Kóspál, Péter Ábrahám, Fernando Cruz-Sáenz de Miera, Eleonora Fiorellino, Michał Siwak, Zsófia Nagy, Teresa Giannini, Roberta Carini, Zsófia Marianna Szabó, Jeong-Eun Lee, Jae-Joon Lee, Fabrizio Vitali, Mária Kun, Borbála Cseh, Máté Krezinger, Levente Kriskovics, András Ordasi, András Pál, Róbert Szakáts, Krisztián Vida, József Vinkó
Figure caption: CO overtone features of Gaia19fct as observed on 2020 November 23. The black line shows the spectrum of Gaia19fct, and the red line represents the best-fit result. The top panel shows the full v = 2 − 0 and v = 3 − 1 series of lines, while the bottom panel is a zoom-in for some of the individual rotational transitions, clearly displaying the emission and two absorption components that make up the spectrum of Gaia19fct.
Paper: The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2
Authors: Jihye Hwang, Jongsoo Kim, Kate Pattle, Chang Won Lee, Patrick M. Koch, Doug Johnstone, Kohji Tomisaka, Anthony Whitworth, Ray S. Furuya, Ji-hyun Kang, A-Ran Lyo, Eun Jung Chung, Doris Arzoumanian, Geumsook Park, Woojin Kwon, Shinyoung Kim, Motohide Tamura, Jungmi Kwon, Archana Soam, Ilseung Han, Thiem Hoang, Kyoung Hee Kim, Takashi Onaka, Chakali Eswaraiah, Derek Ward-Thompson, Hong-Li Liu, Xindi Tang, Wen Ping Chen, Masafumi Matsumura, Thuong Duc Hoang, Zhiwei Chen, Valentin J. M. Le Gouellec, Florian Kirchschlager, Frédérick Poidevin, Pierre Bastien, Keping Qiu, Tetsuo Hasegawa, Shih-Ping Lai, Do-Young Byun, Jungyeon Cho, Minho Choi, Youngwoo Choi, Yunhee Choi, Il-Gyo Jeong, Miju Kang, Hyosung Kim, Kee-Tae Kim, Jeong-Eun Lee, Sang-Sung Lee, Yong-Hee Lee, Hyeseung Lee, Mi-Ryang Kim, Hyunju Yoo, Hyeong-Sik Yun, Mike Chen, James Di Francesco, Jason Fiege, Laura M. Fissel, Erica Franzmann, Martin Houde, Kevin Lacaille, Brenda Matthews, Sarah Sadavoy, Gerald Moriarty-Schieven, Mehrnoosh Tahani, Tao-Chung Ching, Y. Sophia Dai, Yan Duan, Qilao Gu, Chi-Yan Law, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Tie Liu, Xing Lu, Lei Qian, Hongchi Wang, Jintai Wu, Jinjin Xie, Jinghua Yuan, Chuan-Peng Zhang, Guoyin Zhang, Yapeng Zhang, Jianjun Zhou, Lei Zhu, David Berry, Per Friberg, Sarah Graves, Junhao Liu, Steve Mairs, Harriet Parsons, Mark Rawlings, Yasuo Doi, Saeko Hayashi, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Akimasa Kataoka, Koji Kawabata, Gwanjeong Kim, Masato I. N. Kobayashi, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Tae-Soo Pyo, Hiro Saito, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Yusuke Tsukamoto, Tetsuya Zenko, Huei-Ru Vivien Chen, Hao-Yuan Duan, Lapo Fanciullo, Francisca Kemper, Chin-Fei Lee, Sheng-Jun Lin, Sheng-Yuan Liu, Nagayoshi Ohashi, Ramprasad Rao, Ya-Wen Tang, Jia-Wei Wang, Meng-Zhe Yang, Hsi-Wei Yen, Tyler L. Bourke, Antonio Chrysostomou, Victor Debattista, David Eden, Stewart Eyres, Sam Falle, Gary Fuller, Tim Gledhill, Jane Greaves, Matt Griffin, Jennifer Hatchell, Janik Karoly, Jason Kirk, Vera Könyves, Steven Longmore, Sven van Loo, Ilse de Looze, Nicolas Peretto, Felix Priestley, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Giorgio Savini, Anna Scaife, Serena Viti, Pham Ngoc Diep, Nguyen Bich Ngoc, Le Ngoc Tram, Philippe André, Simon Coudé, C. Darren Dowell, Rachel Friesen, Jean-Franćois Robitaille
Figure caption: A map of the angle dispersions of polarization segments. The WK model with i = 30° was used to infer a large-scale mean magnetic field structure in Mon R2. A polarization angle dispersion in a gray pixel is highly uncertain, as a radius of curvature within the pixel is smaller than the size of box (see Appendix B). Contours are the same as those defined in Figure 3.
Paper: The JCMT BISTRO Survey: A Spiral Magnetic Field in a Hub-filament Structure, Monoceros R2
Authors: Jihye Hwang, Jongsoo Kim, Kate Pattle, Chang Won Lee, Patrick M. Koch, Doug Johnstone, Kohji Tomisaka, Anthony Whitworth, Ray S. Furuya, Ji-hyun Kang, A-Ran Lyo, Eun Jung Chung, Doris Arzoumanian, Geumsook Park, Woojin Kwon, Shinyoung Kim, Motohide Tamura, Jungmi Kwon, Archana Soam, Ilseung Han, Thiem Hoang, Kyoung Hee Kim, Takashi Onaka, Chakali Eswaraiah, Derek Ward-Thompson, Hong-Li Liu, Xindi Tang, Wen Ping Chen, Masafumi Matsumura, Thuong Duc Hoang, Zhiwei Chen, Valentin J. M. Le Gouellec, Florian Kirchschlager, Frédérick Poidevin, Pierre Bastien, Keping Qiu, Tetsuo Hasegawa, Shih-Ping Lai, Do-Young Byun, Jungyeon Cho, Minho Choi, Youngwoo Choi, Yunhee Choi, Il-Gyo Jeong, Miju Kang, Hyosung Kim, Kee-Tae Kim, Jeong-Eun Lee, Sang-Sung Lee, Yong-Hee Lee, Hyeseung Lee, Mi-Ryang Kim, Hyunju Yoo, Hyeong-Sik Yun, Mike Chen, James Di Francesco, Jason Fiege, Laura M. Fissel, Erica Franzmann, Martin Houde, Kevin Lacaille, Brenda Matthews, Sarah Sadavoy, Gerald Moriarty-Schieven, Mehrnoosh Tahani, Tao-Chung Ching, Y. Sophia Dai, Yan Duan, Qilao Gu, Chi-Yan Law, Dalei Li, Di Li, Guangxing Li, Hua-bai Li, Tie Liu, Xing Lu, Lei Qian, Hongchi Wang, Jintai Wu, Jinjin Xie, Jinghua Yuan, Chuan-Peng Zhang, Guoyin Zhang, Yapeng Zhang, Jianjun Zhou, Lei Zhu, David Berry, Per Friberg, Sarah Graves, Junhao Liu, Steve Mairs, Harriet Parsons, Mark Rawlings, Yasuo Doi, Saeko Hayashi, Charles L. H. Hull, Tsuyoshi Inoue, Shu-ichiro Inutsuka, Kazunari Iwasaki, Akimasa Kataoka, Koji Kawabata, Gwanjeong Kim, Masato I. N. Kobayashi, Tetsuya Nagata, Fumitaka Nakamura, Hiroyuki Nakanishi, Tae-Soo Pyo, Hiro Saito, Masumichi Seta, Yoshito Shimajiri, Hiroko Shinnaga, Yusuke Tsukamoto, Tetsuya Zenko, Huei-Ru Vivien Chen, Hao-Yuan Duan, Lapo Fanciullo, Francisca Kemper, Chin-Fei Lee, Sheng-Jun Lin, Sheng-Yuan Liu, Nagayoshi Ohashi, Ramprasad Rao, Ya-Wen Tang, Jia-Wei Wang, Meng-Zhe Yang, Hsi-Wei Yen, Tyler L. Bourke, Antonio Chrysostomou, Victor Debattista, David Eden, Stewart Eyres, Sam Falle, Gary Fuller, Tim Gledhill, Jane Greaves, Matt Griffin, Jennifer Hatchell, Janik Karoly, Jason Kirk, Vera Könyves, Steven Longmore, Sven van Loo, Ilse de Looze, Nicolas Peretto, Felix Priestley, Jonathan Rawlings, Brendan Retter, John Richer, Andrew Rigby, Giorgio Savini, Anna Scaife, Serena Viti, Pham Ngoc Diep, Nguyen Bich Ngoc, Le Ngoc Tram, Philippe André, Simon Coudé, C. Darren Dowell, Rachel Friesen, Jean-Franćois Robitaille
Figure caption: Magnetic field angles, Φ B , as a function of azimuthal angle, AZ. The magnetic field and azimuthal angles are measured from west to north with respect to the origin at the position of IRS 1. The colored dots mark our polarization observations, and are color coded by total intensity. The color bar shows the mapping between color and total intensity. The red lines show magnetic field angles estimated using the best-fit WK model. When AZ is between 100° and 150°, offsets between the observations and the best-fit WK model are apparent.